Relations between coronal shock waves properties and acceleration of solar energetic particles
- 1IRAP, CNRS, Université Toulouse III–Paul Sabatier, Toulouse, France (manon.jarry@irap.omp.eu)
- 2Applied Physics Laboratory, The Johns Hopkins University, Laurel, MD, United States
- 3Leibniz-Institut für Astrophysik Potsdam (AIP), Potsdam, Germany
The mechanisms that produce solar energetic particles (SEPs) are still highly debated but coronal shock waves have been proposed as efficient particle accelerators that may be implicated in the production of SEPs.
An analysis of 32 Coronal Mass Ejections (CMEs) that produced strong pressure waves in the solar corona during their eruption has been done. For each event Kouloumvakos et al. (2019) exploited remote-sensing observations from multiple vantage points to reconstruct their 3-D ellipsoidal shapes. This catalogue of shock waves provides important statistical information on their kinematic evolution that we report in Jarry et al. (2023) together with their relation to X-ray flaring activitiy.
Different SEPs exhibit significant spectral and compositional variability. We looked for links between the composition of SEPs including abundance ratios (such as Fe/O) and shock parameters (Mach number, shock geometry, ..) that typically evolves rapidly along the magnetic field lines connected to the spacecraft recording SEPs.
This work was funded by the H2020 SERPENTINE project.
How to cite: Jarry, M., Rouillard, A., Plotnikov, I., Kouloumvakos, A., and Warmuth, A.: Relations between coronal shock waves properties and acceleration of solar energetic particles, EGU General Assembly 2023, Vienna, Austria, 24–28 Apr 2023, EGU23-6946, https://doi.org/10.5194/egusphere-egu23-6946, 2023.
